Neutron stars with a stable, light supersymmetric baryon

Shmuel Balberg, Glennys R. Farrar, Tsvi Piran

    Research output: Contribution to journalArticle

    Abstract

    If a light gluino exists, the lightest gluino-containing baryon, S0, is a possible candidate for self-interacting dark matter. In this scenario, the simplest explanation for the observed ratio ΩDMb ≈ 6 - 10 is that mS0 ≃ 900 MeV c-2; at present, this is not excluded by particle physics. Such an S0 could be present in neutron stars, with the hyperon formation serving as an intermediate stage. We calculate equilibrium compositions and the equation of state for high-density matter with S0, and we find that for a wide range of parameters, the properties of neutron stars with S0 are consistent with observations. In particular, the maximum mass of a nonrotating star is 1.7 - 1.8 M⊙, and the presence of S0 is helpful in reconciling observed cooling rates with hyperon formation.

    Original languageEnglish (US)
    Pages (from-to)L179-L182
    JournalAstrophysical Journal
    Volume548
    Issue number2 PART 2
    DOIs
    StatePublished - Feb 20 2001

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    Keywords

    • Dark matter
    • Dense matter
    • Elementary particles
    • Equation of state
    • Stars: neutron

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

    Cite this

    Balberg, S., Farrar, G. R., & Piran, T. (2001). Neutron stars with a stable, light supersymmetric baryon. Astrophysical Journal, 548(2 PART 2), L179-L182. https://doi.org/10.1086/319101